Einstein had it... Part LXXVI: Quantum Universes – We don’t need no… an Inflation

Abstract
There are Friedmann–Lemaître–Robertson–Walker (FLRW) vacuum solutions to the Einstein-Field-Equations. These solutions contain intrinsic degrees of freedom, which lead, if “activated”, to the classical Klein-Gordon equations of Quantum Theory. The subsequent evaluation results in a great variety of quantum universes.
With some of these quantized FLRW universes and under suitable parameter settings, we find near-big-bang scenarios with a dramatic increase of the effective speed of light in vacuum. Such a development near t=0 would explain the homogeneity of the universe without the need of an inflation theory.
In addition, we quite naturally obtain quantum fluctuations to the early universe (with very first simple calculations) which might provide a suitable explanation for the miniscule inhomogeneity of the cosmological background radiation.
Thus, the paper provides an explanation for the cosmologic homogeneity and the seeds of diversity, which resided in the early universe, leading to all its later structures, without the need of any postulation. Instead only the quantization directly evolving from the Einstein-Hilbert action itself and the use of its intrinsic degrees of freedom gives all the necessary ingredients.